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Ancient and primordial collisional families as the main sources of X-type asteroids of the inner main belt Marco Delbo, Chrysa Avdellidou, Alessandro Morbidelli To cite this version: Marco Delbo, Chrysa Avdellidou, Alessandro Morbidelli. Ancient and primordial collisional families as the main sources of X-type asteroids of the inner main belt. Astronomy and Astrophysics - A&A, EDP Sciences, 2019, 624, pp.A69. 10.1051/0004-6361/201834745. hal-02303454 HAL Id: hal-02303454 https://hal.archives-ouvertes.fr/hal-02303454 Submitted on 19 Aug 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. A&A 624, A69 (2019) Astronomy https://doi.org/10.1051/0004-6361/201834745 & © M. Delbo et al. 2019 Astrophysics Ancient and primordial collisional families as the main sources of X-type asteroids of the inner main belt? Marco Delbo1, Chrysa Avdellidou1,2, and Alessandro Morbidelli1 1 Observatoire de la Côte d’Azur, CNRS–Lagrange, Université Côte d’Azur, CS 34229, 06304 Nice Cedex 4, France e-mail: [email protected] 2 Science Support Office, Directorate of Science, European Space Agency, Keplerlaan 1, 2201 AZ Noordwijk ZH, The Netherlands Received 29 November 2018 / Accepted 26 January 2019 ABSTRACT Aims. The near-Earth asteroid population suggests the existence of an inner main belt source of asteroids that belongs to the spec- troscopic X complex and has moderate albedos. The identification of such a source has been lacking so far. We argue that the most probable source is one or more collisional asteroid families that have escaped discovery up to now. Methods. We apply a novel method to search for asteroid families in the inner main-belt population of asteroids belonging to the X complex with moderate albedo. Instead of searching for asteroid clusters in orbital element space, which could be severely dispersed when older than some billions of years, our method looks for correlations between the orbital semimajor axis and the inverse size of asteroids. This correlation is the signature of members of collisional families that have drifted from a common centre under the effect of the Yarkovsky thermal effect. Results. We identify two previously unknown families in the inner main belt among the moderate-albedo X-complex asteroids. One of them, whose lowest numbered asteroid is (161) Athor, is 3 Gyr old, whereas the second one, whose lowest numbered object is (689) Zita, could be as old as the solar system. Members of∼ this latter family have orbital eccentricities and inclinations that spread them over the entire inner main belt, which is an indication that this family could be primordial, that is, it formed before the giant planet orbital instability. Conclusions. The vast majority of moderate-albedo X-complex asteroids of the inner main belt are genetically related, as they can be included into a few asteroid families. Only nine X-complex asteroids with moderate albedo of the inner main belt cannot be included in asteroid families. We suggest that these bodies formed by direct accretion of the solids in the protoplanetary disc, and are thus surviving planetesimals. Key words. minor planets, asteroids: general – astronomical databases: miscellaneous 1. Introduction However, family members disperse with time. Dispersion is driven by a change in the a-value (da/dt , 0) due to the ther- Collisions in the asteroid main belt are responsible for sculpting mal radiation force of the Yarkovsky effect (Vokrouhlický et al. the size distribution of these bodies (Bottke et al. 2015a), form- 2006); the eccentricity and inclination are affected by orbital ing craters on their surfaces, producing fresh regolith (Hörz & resonances with the planets, the locations of which are crossed Cintala 1997; Basilevsky et al. 2015), ejecting asteroid material by the asteroids as they drift in semimajor axis. This process into space (Jewitt et al. 2011), and also implanting exogenous has fundamental consequences: families older than 2 Gyr tend materials (McCord et al. 2012; Avdellidou et al. 2018, 2017, to lose number density contrast with respect to the∼ local back- 2016; Turrini et al. 2016; Vernazza et al. 2017). ground population (Parker et al. 2008; Spoto et al. 2015; Carruba The most energetic impacts can eject asteroid fragments at et al. 2016). They become more difficult to detect using the HCM speeds larger than the gravitational escape velocity of the parent compared to younger ones (Walsh et al. 2013; Bolin et al. 2017; body. This process can form families of daughter asteroids ini- Delbo et al. 2017). In addition to the effect of orbital resonances tially placed on orbits that group near that of the parent asteroid currently present in the main belt, the scattering of fragments of (Zappala et al. 1984). Asteroid families can therefore be recog- primordial families (Milani et al. 2017, 2014; Delbo et al. 2017) nised as clusters of bodies in proper orbital element space – was also affected by major dynamical events such as the giant proper semimajor axis, proper eccentricity, and proper inclina- planet orbital instability, which is shown to have happened at tion (a; e; i) – with significant contrast with respect to the local some point in the solar system history (Morbidelli et al. 2015). background (Milani et al. 2014; Nesvorný et al. 2015). The hier- This latter instability shifted the positions of the resonances and archical clustering method (HCM; Zappalà et al. 1990; Nesvorný resulted in the incoherent dispersion of e and i of any pre-existing et al. 2015, and references therein) is typically used for the primordial asteroid family in the main belt (Brasil et al. 2016), as identification of these asteroid clusters. is the case for the family of low-albedo asteroids found by Delbo et al.(2017) in the inner main belt (i.e. 2.1 < a < 2.5 au). ? This work is dedicated to the memory of Andrea Milani, who put The sign of da/dt depends on the obliquity of the spin vec- the foundation and devoted his scientific career on the study of asteroid tor of the asteroid, with prograde-rotating asteroids drifting with families. da/dt > 0 and retrograde ones with da/dt < 0. To first order, the A69, page 1 of 21 Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. A&A 624, A69 (2019) value of da/dt is inversely proportional to the diameter D of fam- diameter. This means that the smaller low-albedo asteroids of the ily members, such that at any given epoch, the orbits of smaller inner main belt could be genetically linked to a few distinct aster- asteroids are moved further away from the centre of the fam- oid parents (Delbo et al. 2017) and that the low-albedo NEAs ily than the bigger ones are. Due to this mechanism, an asteroid with a high probability of coming from the inner main belt are family forms a characteristic shape in the space of proper semi- also linked to these few distinct asteroid parents. These later find- major axis a versus inverse diameter (a; 1=D), which is called ings are also independently confirmed by the work of Dermott V-shape as the distribution of asteroids resembles the letter “V” et al.(2018). (Milani et al. 2014; Spoto et al. 2015; Bolin et al. 2017). The On the other hand, concerning the NEAs with high albedo slopes of the borders of the “V” indicate the age of a family (pV > 0:12) and not those belonging to the spectroscopic (see e.g. Spoto et al. 2015), with younger ones having steeper C-complex, the situation is less clear. Nonetheless, several and older ones shallower slopes. While orbital resonance cross- important S-complex families in the inner main belt are known ings produce diffusion of e and i; these have minimal effect on a that could be the source of NEAs belonging to the same spectro- (Milic´ Žitnik & Novakovic´ 2016), resulting in the conservation scopic complex. For instance, the Flora family (Vernazza et al. of the V-shape of families for billions of years. The semimajor 2008) is capable of delivering NEAs belonging to the S com- axis values can only be modified by gravitational scattering due plex and with composition similar to the LL ordinary chondrite to close encounters with massive asteroids (Carruba et al. 2013; meteorites (Vokrouhlický et al. 2017). Moreover, Reddy et al. Delisle & Laskar 2012) or in the case that a planet momentar- (2014) propose that the Baptistina asteroid family is the source of ily entered the main belt during the orbital instability phases of LL chondrites that show shock-blackened impact melt material. the giant planets (Brasil et al. 2016). The former effect has been The NEA population also contains a significant number of shown to be negligible for families with ages of approximately X-complex asteroids (Binzel et al. 2015), whose origin remains 1 Gyr (Delbo et al. 2017). The second case did not happen for the unclear despite their link with meteorites and asteroids being inner main belt; if it had, the V-shape of the primordial family visited by space missions (see Sect.2).

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